# The Co-Evolution of a Magnetized Intracluster Medium and Hot Galactic Coronae: Magnetic Field Amplification and Turbulence Generation

## TL;DR

This study uses magnetohydrodynamic simulations to explore how galaxies influence magnetic fields and turbulence in the intracluster medium, revealing magnetic field amplification, turbulence generation, and observable effects in Faraday rotation maps.

## Contribution

It demonstrates the role of orbiting galaxies in amplifying magnetic fields and generating turbulence in the ICM, highlighting effects on magnetic morphology and potential observational signatures.

## Key findings

- Magnetic fields are draped and aligned with galaxy tails, affecting their morphology.
- Galaxies amplify magnetic fields and inject turbulence into the ICM.
- Turbulent kinetic energy increases temporarily but does not dominate the ICM energy budget.

## Abstract

We use adaptive-mesh magnetohydrodynamic simulations to study the effect of magnetic fields on ram pressure stripping of galaxies in the intracluster medium (ICM). Although the magnetic pressure in typical clusters is not strong enough to affect the gas mass loss rate from galaxies, magnetic fields can affect the morphology of stripped galaxies. ICM magnetic fields are draped around orbiting galaxies and aligned with their stripped tails. Magnetic fields suppress shear instabilities at the galaxy-ICM interface, and magnetized tails are smoother and narrower than tails in comparable hydrodynamic simulations in Vijayaraghavan & Ricker (2015). Orbiting galaxies stretch and amplify ICM magnetic fields, amplifying magnetic power spectra on $10 - 100$ kpc scales. Galaxies inject turbulent kinetic energy into the ICM via their turbulent wakes and $g$-waves. The magnetic energy and kinetic energy in the ICM increase up to $1.5 - 2$ Gyr of evolution, after which galaxies are stripped of most of their gas, and do not have sufficiently large gaseous cross sections to further amplify magnetic fields and inject turbulent kinetic energy. The increase in turbulent pressure due to galaxy stripping and generation of $g$-waves results in an increase in the turbulent volume fraction of the ICM. This turbulent kinetic energy is not a significant contributor to the overall ICM energy budget, but greatly impacts the evolution of the ICM magnetic field. Additionally, the effect of galaxies on magnetic fields can potentially be observed in high resolution Faraday rotation measure (RM) maps as small scale fluctuations in the RM structure.